Observation method
The solar images in the HeI 1083nm line are obtaining with the aid of the telescope TST-2of the Crimean Astrophysical Observatory. They are obtained due scan toning
of the Sun images through the slit of the spectrograph. The photometer detects the
intensity in the center of the HeI 1083nm line. The telescope and detecting device are
served by PC/AT 386 computer. The time of observation and space resolution ix, iy are
given in the observation list. All images presented at the page are normalized to 9.8x9.8
arc sec per pixel. The equator direction is approximately horizontal. Right images are
corrected for limb darkening and left ones are not corrected.The archive of images in the HeI 1083nm line is here.

Observation method
The coronagraph-1 (KG-1) was designed by the State Optical and Mechanical Plant according
to the Lyot layout and put into operation in 1951. Positioned on the equatorial mounting,
it is a refractor with the 21-cm objective. The objective is made of glass K8. It is a
convex-plane lens 10 mm thick with the 350-cm focal length in the H-alpha 6562.8 Å line.
The telescope is used for chromospheric monochromatic observations of prominences,
filaments, active regions and flares in the H-alpha line. In the focal plane of the
objective there is a diaphragm cutting out a part of the solar image. Next to the
diaphragm there is another objective. Passing through it, a beam becomes parallel. Then
light falls on the diagonal mirror and interference-polarization filter (IPF). After IPF
light goes to the diagonal mirror, then to the lens of the field, and depending on the
rotary motion of the third diagonal mirror, either to the ocular or to the digital camera.
The focal length of this layout is 7 meters. The 12-cm image of the Sun is built up in the
focal plane. Optical resolution of the telescope is 1.5.

Observations
An image of a part of the solar disk (3888 õ 2592 pixels or 355.5 õ 266.6 angular
seconds in size) is taken with the digital camera. The image is oriented across the
diurnal circle. Observations are carried out in the center and in wings of the H-alpha
active regions and filaments on the solar disk, as well as prominences on the limb.

Observation method
Visual measurements of sunspot magnetic fields are carrying out in the Crimean Astrophysical Observatory from 1955. First two years the line
FeI 6173 A was used. Since 1957 observations are carrying out in the line FeI 6302 A.
Maximal distance between sigma-components is measured in the profile of this line splitted
in a sunspot magnetic field. Then the measured size is transferred in intensity of a
magnetic field.
The data of observations of each day are presented in a kind of sketch of the solar disk
with all sunspot groups and their temporary numbers. Near each sunspot the sign of
magnetic field ( N or S) and intensity in hundreds Gauss is specified. The moment of
observation (UT), quality of the image (seeing) in five step scale and scintillation
(Scintillation) in arc seconds is specified above the sketch. The line EW corresponds to a
direction of an equator.The archive of sunspot magnetic fields is here.

These data involve
areas of sunspot groups and intensity distribution of the HeI 1083 nm line across the
solar surface for each rotation of the Sun.
The areas of sunspot groups are detected based on sketches in white light of the
110-mm-diameter Sun's disk.
The HeI line intensity is determined by scanning the solar disk with a multi-purpose
spectrophotometer.
The maps being built taking into account solar limb darkening and normalized to a unit are
filled with isophotes 0.9 typical for brightness in active regions and filaments and 1.02
typical for coronal holes.
The region defined by isophote 0.9 is marked in yellow and defined by isophote 1.02 - in
brown.

The position of sunspot groups for each observation day is indicated on the synoptic maps.
The area of a group is represented by a rectangle, lengths of sides are equal to
longitudinal and
latitudinal
extension of the sunspot group. Individual sunspots are represented by dots.

Two vertical dashed lines correspond to the starting and ending
of the Carrington rotation. Dashes directed downward along the x axis
indicate longitudes of the central meridian (Lo) in moments of observations.The archive of synoptic maps is here.